Aperture photometry using APT

Downloading, Installing, and Starting the Software

APT = Aperture Photometry Tool. Russ Laher wrote it, and it can be downloaded here. Follow the directions there to install it. You may be interested in the Unix cheatsheet. If you're using windows, see the windows hints, tips, and tricks page.

For Macs, I found that I needed to start it from the command line (terminal window) in the Applications directory where I installed it. I couldn't start it by double-clicking on the icon.

For a comprehensive introduction to APT, please see this page. The stuff that is here on the wiki is more skeletal, and is likely out of date with respect to screen grabs, etc.

Loading an image

Click on "choose FITS image" and load an image. It will come up with a default stretch. You can use the buttons and fill-in boxes to change the stretch (limits and scale) if desired. You can obtain a histogram of the values in the image by clicking on the "image histogram" button.

Picking an object, Doing the photometry, and Exploring the options

Use your mouse, scroll around in the image in the upper right, and find an object you wish to measure. Click on the object. In the lower center of the APT window, it gives you a greatly magnified version of the portion of the image you are investigating. You should use this zoom-in to try to center your object on the mouse cursor as accurately as possible - the better your initial guess, the easier it will be for the computer to correctly centroid the object.

The program did the photometry using its default values. The centroid radius (e.g., the max offset that it can calculate the centroid from your initial guess), the aperture radius, and the sky annulus parameters (inner and outer sky radius) are all set to particular values by default. They are in units of pixels. To figure out what these values are in arcseconds, look at the FITS header for your image. Click on "show FITS header" (top center), and find CDELT1 or CDELT2. These are the numbers of degrees per pixel. Convert this value to arcseconds by mulitplying by 3600 arcseconds/degree. Make sure that the aperture and annulus parameters are what you want them to be. (See this page for more discussion.)

You can use the following buttons to further explore your choice of aperture and annulus size. In each case, the aperture and annulus sizes are indicated, along with its calculated background level:

• aperture slice - one-dimensional slice through the aperture. Allows you to investigate if the source is resolved or saturated.
• curve of growth - how the total flux measured changes as a function of aperture
• source scatter - range of pixel values within the aperture -- you can explore the effects of too large or small an aperture here.
• radial profile - circularly averaged slice through the aperture. The PSF is circularly symmetric, so this allows you to explore the placement of the annulus (is it on top of the Airy ring?) and the level of the background more easily than the aperture slice option above. This also allows you to investigate whether the source is resolved or saturated.
• sky scatter - range of pixel values within the sky annulus -- you can explore the effects of too large or small an annulus, or the influence of nearby sources or nebulosity, here.
• sky histogram - histogram of pixel values within the sky annulus -- you can explore the effects of too large or small an annulus, or the influence of nearby sources or nebulosity, here.
• hide/show aperture - should be obvious what this means!
• color table toggle - changes the color table

If you change any of the values, you will need to ask it to 'recompute photometry' (button in the lower left). Changes in the requested aperture/annulus will be reflected in the display indicating the size of the annulus/aperture in the lower right, as well as in all the popup graphs you can get from clicking on the buttons described above.

The results of the photometry are reported under "RESULTS" in the lower left. Note that it recognizes the units of your input image (MJy/sr, DN, whatever) and reports the photometry in the same units. Review the information on Spitzer units, specifically as it applies to units of Spitzer images. In order to get it to report the photometry in Jy, instead of MJy/sr, you will need to derive the appropriate image data unit conversion factor, and corresponding reasonable units after conversion -- there's information on this on the Units page. Then go to "more settings" and enter those values in the corresponding boxes. If you click the "perform image data conversion" box, it will report the photometry in Jy (or whatever unit you want) on the main screen.

You can manually keep notes on the photometry you are calculating, or you can click the button that says "save photometry data" to write the values for this object to a file. If you click on "show photometry file", you can see the file it's accumulating. Note that as of this time, it does NOT tabulate RA/Dec. Russ is working on that, and this feature will be in a future version.